In the studied spectral range, there are multiple forbidden emission lines associated with outflowing material from young stars [1]}, [2]}, [3]}. Present in these data with a strong S/N are the [Oi] 6300 Å and [Sii] 6730 Å emission lines. The flux calibrated spectra of these lines from the 12 epochs can be seen in Fig. REF . The vast majority of the emission from the [Oi] 6300 Å line is blue-shifted and it is completely blue-shifted in the [Sii] 6730 Å. Both lines have a very similar profile with wings reaching very high systematic velocities, namely \(\sim \!-300\)  and \(\sim \!-380\)  km s\(^{-1}\)  for the [Sii] 6730 Å and the [Oi] 6300 Å lines, respectively. These wing velocity values are slightly higher than those found for RU Lup in the observations of [4]} and [5]} in 2008 (\(\sim \!-270\)  km s\(^{-1}\)  for [Oi] 6300 Å) and [6]} in 2012 (\(\sim \!-250\)  and \(\sim \!-280\)  km s\(^{-1}\) , for the [Sii] 6730 Å and the [Oi] 6300 Å lines, respectively). All these values for the wings of the HVC in RU Lup are typically higher than those of other TTS with this forbidden emission, often by at least 100 km s\(^{-1}\) , as can be seen in Figure 17 of [4]} for the case of the [Oi] 6300 Å line.
